An Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas.
George Mason University (USA) -
University of Michigan (USA) -
University of Cambridge (UK)
CHIANTI consists of a critically evaluated set of up-to-date atomic
data, together with user-friendly programs written
in Interactive Data Language (IDL) and Python to calculate the spectra
from astrophysical plasmas.
The CHIANTI package is freely available.
If you use the package, we only ask you to
acknowledge CHIANTI .
- The Chianti wine-producing area of Tuscany, Italy -
CHIANTI Database Version 7.1.3 and the CHIANTI IDL package version 7.1.4 released on August 14, 2013
An error in the routine that calculates radiative recombination rates was discovered. This error mainly affected the ionization fractions of the neutral and first ionization stage. The new database file contains a corrected file of ionization equilibria chianti.ioneq as well as the previous version that has been renamed to chianti_v7.ioneq for those who are interested in the checking the differences.
A plot of the differences between the new and old ionization fractions for oxygen can be found here .
The IDL package contains the updated version of recomb_rate.pro with the corrected calculation of the recombination rate. The ChiantiPy is already correct in this aspect.
CHIANTI Version 7.1.2 released on May 23, 2013
Version 7.1.1 is a bug-fix release. It corrects problems with the o_2.wgfa file that contains wavelengths, weighted-oscillator strengths and A-values.
CHIANTI Version 7.1.1 released on April 30, 2013
Version 7.1.1 is a bug-fix release. It corrects problems with the c_2.wgfa file that contains wavelengths, weighted-oscillator strengths and A-values.
CHIANTI Version 7.1 released
The main feature of CHIANTI Version 7.1 is the inclusion of a large
number of configurations to the atomic models of Fe VIII to XIV. These
configurations give rise to a forest of spectral lines in the 50-170 A
wavelength range that contribute significantly to the total radiative
output of the Sun at those wavelengths. Also, they give rise to several
strong lines that are currently neglected by spectral codes, and provide
significant contributions to the SDO/AIA bandpasses centered at 94A
and 131A. These data are calculated using the Flexible Atomic Code
(FAC) under the distorted wave approximation.
Additional data for a few more ions are included, that improve
the available datasets for a few ions, and correct a few glitches for
other ions at all wavelength ranges. New element abundance data
sets are provided, and improved recombination rates are included
and used to provide a new set of CHIANTI ionization equilibria
We are grateful to
individual scientists and funding agencies for their support.